The physics and chemistry of the L134N molecular core

Details The physics and chemistry of the L134N molecular core The physics and chemistry of the L134N molecular core

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345..828s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 345, Oct. 15, 1989, p. 828-852.

Physics

105

Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Molecular Physics, Nebulae, Abundance, Ammonia, Carbon Monoxide, Hyperfine Structure, Isotopes, Sulfides

Scientific paper

The dark cloud L134N is studied in detail via millimeter- and centimeter-wavelength emission-line spectra. A high-density core of molecular gas exists in L134N which has a kinetic temperature of about 12 K, a peak molecular hydrogen density of about 10 exp 4.5/cu cm, and a mass of about 23 solar. The core may be the site of future star formation. Maps of emission from (C-18)O, CS, H(C-13)O(+), SO, NH3, and C3H2 reveal morphologically different distributions resulting in part from both varying physical conditions within the cloud and optical depth effects. Significant differences also exist which are probably due to chemical abundance variations. A consistent set of LTE chemical abundances has been estimated at as many as seven positions, which can be used to constrain chemical models of dark clouds.

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